Stellar Physics
PHYS 501 · Module 2
This module explains how stars form, shine, and evolve. Students study hydrostatic equilibrium, nuclear fusion, the Hertzsprung-Russell diagram, and the life cycles of stars of different masses.
Lessons in this module
Stellar structure and hydrostatic equilibrium
Stars are stable for long periods because pressure gradients balance gravity. This lesson introduces hydrostatic equilibrium, mass conservation, energy transport, and stellar structure equations.
Nuclear fusion in stars
Stars shine by converting nuclear mass into energy. This lesson explains Coulomb barriers, quantum tunneling, the proton-proton chain, the CNO cycle, and stellar energy generation.
The Hertzsprung-Russell diagram
The Hertzsprung-Russell diagram organizes stars by luminosity and temperature. This lesson explains the main sequence, giants, white dwarfs, stellar radii, and evolutionary tracks.
Stellar evolution from birth to death
A star's life is controlled mainly by its mass. This lesson follows stars from molecular clouds to protostars, main-sequence life, red giant phases, supernovae, and stellar remnants.
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